Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 1 1.Newton’s Law of Universal Gravitation 2.Kepler’s Laws 3.Motion in Accelerated Frames PHYS 1443 – Section 003 Lecture #11 Monday, Oct. 4, 2004 Dr. Jaehoon Yu

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 2 Newton’s Law of Universal Gravitation People have been very curious about stars in the sky, making observations for a long time. But the data people collected have not been explained until Newton has discovered the law of gravitation. Every particle in the Universe attracts every other particle with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them. How would you write this law mathematically? G is the universal gravitational constant, and its value is This constant is not given by the theory but must be measured by experiments. With G Unit? This form of forces is known as the inverse-square law, because the magnitude of the force is inversely proportional to the square of the distances between the objects.

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 3 It means that the force exerted on the particle 2 by particle 1 is an attractive force, pulling #2 toward #1. More on Law of Universal Gravitation Consider two particles exerting gravitational forces to each other. Gravitational force is a field force: Forces act on object without physical contact between the objects at all times, independent of medium between them. The gravitational force exerted by a finite size, spherically symmetric mass distribution on an object outside of it is the same as when the entire mass of the distributions is concentrated at the center of the object. m1m1 m2m2 r F 21 F 12 Two objects exert gravitational force on each other following Newton’s 3 rd law. Taking as the unit vector, we can write the force m 2 experiences as What do you think the negative sign mean? What do you think the gravitational force on the surface of the earth look?

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 4 Example for Gravitation Using the fact that g=9.80m/s 2 at the Earth’s surface, find the average density of the Earth. Since the gravitational acceleration is Therefore the density of the Earth is Solving for ME

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 5 Free Fall Acceleration & Gravitational Force Weight of an object with mass m is mg. Using the force exerting on a particle of mass m on the surface of the Earth, one can obtain The gravitational acceleration is independent of the mass of the object The gravitational acceleration decreases as the altitude increases If the distance from the surface of the Earth gets infinitely large, the weight of the object approaches 0. What would the gravitational acceleration be if the object is at an altitude h above the surface of the Earth? What do these tell us about the gravitational acceleration? Distance from the center of the Earth to the object at the altitude h.

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 6 Example for Gravitational Force The international space station is designed to operate at an altitude of 350km. When completed, it will have a weight (measured on the surface of the Earth) of 4.22x10 6 N. What is its weight when in its orbit? The total weight of the station on the surface of the Earth is Therefore the weight in the orbit is Since the orbit is at 350km above the surface of the Earth, the gravitational force at that height is

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 7 Kepler’s Laws & Ellipse Kepler lived in Germany and discovered the law’s governing planets’ movement some 70 years before Newton, by analyzing data. Newton’s laws explain the cause of the above laws. Kepler’s third law is a direct consequence of law of gravitation being inverse square law. F1F1 F2F2 b c a Ellipses have two different axis, major (long) and minor (short) axis, and two focal points, F 1 & F 2 a is the length of a semi-major axis b is the length of a semi-minor axis 1.All planets move in elliptical orbits with the Sun at one focal point. 2.The radius vector drawn from the Sun to a planet sweeps out equal area in equal time intervals. ( Angular momentum conservation ) 3.The square of the orbital period of any planet is proportional to the cube of the semi-major axis of the elliptical orbit.

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 8 The Law of Gravity and Motions of Planets Newton assumed that the law of gravitation applies the same whether it is on the Moon or the apple on the surface of the Earth. The interacting bodies are assumed to be point like particles. Therefore the centripetal acceleration of the Moon, a M, is Newton predicted that the ratio of the Moon’s acceleration a M to the apple’s acceleration g would be RERE Moon Apple g aMaM v Newton also calculated the Moon’s orbital acceleration a M from the knowledge of its distance from the Earth and its orbital period, T=27.32 days=2.36x10 6 s This means that the Moon’s distance is about 60 times that of the Earth’s radius, and its acceleration is reduced by the square of the ratio. This proves that the inverse square law is valid.

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 9 Kepler’s Third Law It is crucial to show that Keper’s third law can be predicted from the inverse square law for circular orbits. Since the orbital speed, v, of the planet with period T is Since the gravitational force exerted by the Sun is radially directed toward the Sun to keep the planet on a near circular path, we can apply Newton’s second law The above can be written This is Kepler’s third law. It’s also valid for ellipse for r being the length of the semi-major axis. The constant K s is independent of mass of the planet. v r Solving for T one can obtain and

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 10 Example of Kepler’s Third Law Calculate the mass of the Sun using the fact that the period of the Earth’s orbit around the Sun is 3.16x10 7 s, and its distance from the Sun is 1.496x10 11 m. Using Kepler’s third law. The mass of the Sun, M s, is

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 11 Kepler’s Second Law and Angular Momentum Conservation Since the gravitational force acting on the planet is always toward radial direction, it is a central force Consider a planet of mass M p moving around the Sun in an elliptical orbit. Because the gravitational force exerted on a planet by the Sun results in no torque, the angular momentum L of the planet is constant. This is Keper’s second law which states that the radius vector from the Sun to a planet sweeps our equal areas in equal time intervals. Therefore the torque acting on the planet by this force is always 0. Since torque is the time rate change of angular momentum L, the angular momentum is constant. S B A D C r dr Since the area swept by the motion of the planet is

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 12 Motion in Accelerated Frames Newton’s laws are valid only when observations are made in an inertial frame of reference. What happens in a non-inertial frame? Fictitious forces are needed to apply Newton’s second law in an accelerated frame. This force does not exist when the observations are made in an inertial reference frame. What does this mean and why is this true? Let’s consider a free ball inside a box under uniform circular motion. We see that the box has a radial force exerted on it but none on the ball directly How does this motion look like in an inertial frame (or frame outside a box)? r FrFr How does this motion look like in the box? The ball is tumbled over to the wall of the box and feels that it is getting force that pushes it toward the wall. Why? According to Newton’s first law, the ball wants to continue on its original movement but since the box is turning, the ball feels like it is being pushed toward the wall relative to everything else in the box. v

Monday, Oct. 4, 2004PHYS , Fall 2004 Dr. Jaehoon Yu 13 Non-Inertial Frame Example of Motion in Accelerated Frames A ball of mass m is hung by a cord to the ceiling of a boxcar that is moving with an acceleration a. What do the inertial observer at rest and the non-inertial observer traveling inside the car conclude? How do they differ? m This is how the ball looks like no matter which frame you are in. Inertial Frame  How do the free-body diagrams look for two frames? Fg=mgFg=mg m  T Fg=mgFg=mg m  T F fic acac How do the motions interpreted in these two frames? Any differences? For an inertial frame observer, the forces being exerted on the ball are only T and F g. The acceleration of the ball is the same as that of the box car and is provided by the x component of the tension force. In the non-inertial frame observer, the forces being exerted on the ball are T, F g, and F fic. For some reason the ball is under a force, F fic, that provides acceleration to the ball. While the mathematical expression of the acceleration of the ball is identical to that of inertial frame observer’s, the cause of the force is dramatically different.